Possible detection of flare-generated positrons by HELIOS 1 on 3 Jun 1982

Details Possible detection of flare-generated positrons by HELIOS 1 on 3 Jun 1982 Possible detection of flare-generated positrons by HELIOS 1 on 3 Jun 1982

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4..158k&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 158-161 (SEE N85-34729 23-92)

Computer Science

Gamma Rays, Interplanetary Space, Positrons, Solar Flares, Charged Particles, Compton Effect, Line Spectra, Photosphere, Positron Annihilation

Scientific paper

The production of neutrons and gamma-ray lines by solar particles in the photosphere has been studied. The principal positron emiters which lead to the 0.51 MeV gamma-line are C-11 0-14, 0-15, N-13, Ne-19. The energies of the positrons form radioactive nuclei are of the order of few hundred keV. Positrons resulting from the pi(+) decay have energies of approx 10-100 MeV and cannot be measured by the MPAe-detector. Most of the positrons annihilate in the photosphere. A fraction however should be able to escape into the interplanetary space. Proton, electron and , for the first time, positron measurements (E = 152-546 keV) obtained by the MPAe-particle detector on board of Helios 1 are presented.

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